The reactions 13C( ; n)16O and 22Ne( ; n)25Mg are the primary sources of neutrons for the astrophysical s-process. The feasibility of cross section measurements within the respective Gamow windows is discussed in quantitative terms for a 4 neutron counter, based on 3He tubes and a neutron moderator, placed in an underground lab.
The reactions 13C(; n)16O and 22Ne(; n)25Mg are the primary sources of neutrons for the astrophysical s-process. The feasibility of cross section measurements within th...

The reactions 13C( ; n)16O and 22Ne( ; n)25Mg are the primary sources of neutrons for the astrophysical s-process. The feasibility of cross section measurements within the respective Gamow windows is discussed in quantitative terms for a 4 neutron counter, based on 3He tubes and a neutron moderator, placed in an underground lab.
The reactions 13C(; n)16O and 22Ne(; n)25Mg are the primary sources of neutrons for the astrophysical s-process. The feasibility of cross section measurements within the respective Gamow windows is discussed in quantitative terms for a 4 neutron counter, based on 3He tubes and a neutron moderator, placed in an underground lab.